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  2. WD J2147–4035 - Wikipedia

    en.wikipedia.org/wiki/WD_J2147–4035

    The white dwarf existed for 10.21 ±0.22 Gyrs, meaning the total age is 10.7 ±0.3 Gyrs. [1] Cold white dwarfs are often strongly affected by collision induced absorption (CIA) of hydrogen. This can lead to faint optical red and infrared brightness. These white dwarfs are also called IR-faint white dwarfs. WD J2147–4035 is however very red (r ...

  3. WD 1145+017 - Wikipedia

    en.wikipedia.org/wiki/WD_1145+017

    The supposed planetesimal, WD 1145+017 b, [13] with a 4.5 hour orbit, is being ripped apart by the star and is a remnant of the former planetary system that the star hosted before becoming a white dwarf. [8] [9] It is the first observation of a planetary object being shredded by a white dwarf. Several other large pieces have been seen in orbit ...

  4. List of exoplanets and planetary debris around white dwarfs

    en.wikipedia.org/wiki/List_of_exoplanets_and...

    About 6% of white dwarfs show infrared excess due to a disk around a white dwarf. [66] In the past only a relative small sample of white dwarf disks was known. [67] Due to advances in white dwarf detection (e.g. with Gaia or LAMOST) and improvement of WISE infrared catalogs with unWISE/CatWISE, the number has increased to hundreds of candidates.

  5. Exoplanet orbital and physical parameters - Wikipedia

    en.wikipedia.org/wiki/Exoplanet_orbital_and...

    In a few cases an apparent exoplanet may be a more massive object such as a brown dwarf or red dwarf. However, the probability of a small value of i (say less than 30 degrees, which would give a true mass at least double the observed lower limit) is relatively low (1− √ 3 /2 ≈ 13%) and hence most planets will have true masses fairly close ...

  6. White dwarf - Wikipedia

    en.wikipedia.org/wiki/White_dwarf

    The red dwarf spirals inwards towards the core and might merge with the core. If this does not happen and instead the common envelope is ejected, then the binary ends up in a close orbit, consisting of a white dwarf and a red dwarf. This type of binary is called a post-common envelope binary.

  7. PHL 5038 - Wikipedia

    en.wikipedia.org/wiki/PHL_5038

    The white dwarf PHL 5038A was discovered in 2006 in data from the Sloan Digital Sky Survey [3] and the brown dwarf companion was discovered in 2009 from UKIDSS infrared excess and confirmed with Gemini North to be a spacially resolved binary. [4] It was only the fourth known brown dwarf to orbit a white dwarf at the time.

  8. List of white dwarfs - Wikipedia

    en.wikipedia.org/wiki/List_of_white_dwarfs

    First white dwarf with a planet WD B1620−26: 2003 PSR B1620-26 b (planet) This planet is a circumbinary planet, which circles both stars in the PSR B1620-26 system [5] [6] First singular white dwarf with a planet WD 1145+017: 2015 WD 1145+017 b: Planet is extremely small and is disintegrating. First white dwarf that is a pulsar: AR Scorpii A ...

  9. HD 49798 - Wikipedia

    en.wikipedia.org/wiki/HD_49798

    It is a white dwarf with about 1.3 solar masses, in orbit about HD 49798 and rotating once every 13 seconds. [11] This is detected from the 13-second X-ray pulse, which results from the stellar wind accreting onto the compact object. [8] It has been proposed that the white dwarf is surrounded by a debris disk.